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Using SDO/HMI and SDO/AIA data for sunspot groups of the 24th solar cycle, weanalyzed magnetic properties and He II 304 emission in leading and followingsunspots separately. Simultaneous examination of umbral magnetic properties andatmospheric characteristics above the umbrae draws on average differences in HeII 304 contrast over the umbrae of leading and following spots we discoveredearlier for solar cycle 23 sunspot groups based on SOHO data as well as on thehypothetical relationship between contrast asymmetry and magnetic fieldasymmetry in umbrae. We use a more accurate and faster algorithm for solvingthe pi-uncertainty problem of the transverse magnetic field direction in thisresearch producing new results on differences in magnetic field propertiesbetween magneto-conjugated leaders and followers. We found that, in ~78% of thecases, the minimum (over the umbra area) angle between the magnetic field lineand the normal to the solar surface, a_min, is smaller in the leading spots, sothe magnetic field there is more vertical than that in the counterpartfollowing spot. It was also found that umbral area-averaged angle <a> in ~83%of the spot groups examined is smaller in the leader compared to the followerand the maximum and mean magnetic flux densities inside the umbra depend on theumbral area.

Leading and following sunspots: their magnetic properties and ultra-violet emission above them